
Stars on the parts of the curve where this criterion is not satisfied, such as those to the left of the maximum mass in Fig. REF , are known to be unstable in GR [1]}. This was also observed to be the case for spontaneous scalarization so far. Once the highest ADM mass is reached in the mass-radius curve, we still obtain scalarized solutions with even higher values of \(\tilde{\rho }_c\) , but lower ADM masses, however, these are unstable as in GR [2]}.
